轧制变形及随后热处理对板条马氏体的影响

本文研究了轧制变形及随后热处理对板条马氏体的影响,结果表明：大变形量的重度轧制可使马氏体板条趋于沿轧向排列,层片致密,马氏体板条厚度缩减至20nm左右,在板厚方向上形成了显微层压板结构。低于350℃长时退火,组织处于回复阶段,马氏体形态与轧后近似;高于350℃退火,组织开始进入再结晶期,并有新晶粒生成。     

组合导航制导系统的容错技术及特点

论述了组合导航制导系统的容错设计方案，其中包括ＩＮＳ／ＧＰＳ（惯性导航／全球定位系统）组合系统容错技术、ＳＩＮＳ／ＧＰＳ／多普勒组合系统的容错技术及ＩＮＳ／ＧＰＳ／ＣＮＳ组合系统的容错技术；然后分析了组合导航制导系统的抗故障问题，给出了组合导航、制导系统的故障分类和系统出故障后的运用情况；最后，对其发展进行了展望，并提出了今后有待进一步研究的问题。     

航空发动机叶片-机匣碰摩摩擦热效应仿真分析

为了分析航空发动机叶片-机匣碰摩摩擦热对叶片的影响,基于有限元法建立了叶片-机匣碰摩摩擦的热-结构直接耦合模型,分析了不同偏心距和转速对模型应力场和温度场的影响,并与未考虑摩擦热效应的碰摩模型进行对比。结果表明:当叶片与机匣之间发生摩擦时,需考虑材料参数随温度变化的影响;摩擦热主要分布在接触表面较小的区域,温度分布沿接触面向四周呈递减趋势,且温度梯度越来越小。并在该区域产生了较大的热应力;随着偏心距和转速的增大,叶片-机匣的摩擦热效应越发明显。在实际工程问题中,需考虑摩擦热效应对叶尖表面损伤的影响。     

Towards a Unified View of Inhomogeneous Stellar Winds in Isolated Supergiant Stars and Supergiant High Mass X-Ray Binaries

Massive stars, at least \(\sim10\) times more massive than the Sun, have two key properties that make them the main drivers of evolution of star clusters, galaxies, and the Universe as a whole. On the one hand, the outer layers of massive stars are so hot that they produce most of the ionizing ultraviolet radiation of galaxies; in fact, the first massive stars helped to re-ionize the Universe after its Dark Ages. Another important property of massive stars are the strong stellar winds and outflows they produce. This mass loss, and finally the explosion of a massive star as a supernova or a gamma-ray burst, provide a significant input of mechanical and radiative energy into the interstellar space. These two properties together make massive stars one of the most important cosmic engines: they trigger the star formation and enrich the interstellar medium with heavy elements, that ultimately leads to formation of Earth-like rocky planets and the development of complex life. The study of massive star winds is thus a truly multidisciplinary field and has a wide impact on different areas of astronomy.In recent years observational and theoretical evidences have been growing that these winds are not smooth and homogeneous as previously assumed, but rather populated by dense “clumps”. The presence of these structures dramatically affects the mass loss rates derived from the study of stellar winds. Clump properties in isolated stars are nowadays inferred mostly through indirect methods (i.e., spectroscopic observations of line profiles in various wavelength regimes, and their analysis based on tailored, inhomogeneous wind models). The limited characterization of the clump physical properties (mass, size) obtained so far have led to large uncertainties in the mass loss rates from massive stars. Such uncertainties limit our understanding of the role of massive star winds in galactic and cosmic evolution.Supergiant high mass X-ray binaries (SgXBs) are among the brightest X-ray sources in the sky. A large number of them consist of a neutron star accreting from the wind of a massive companion and producing a powerful X-ray source. The characteristics of the stellar wind together with the complex interactions between the compact object and the donor star determine the observed X-ray output from all these systems. Consequently, the use of SgXBs for studies of massive stars is only possible when the physics of the stellar winds, the compact objects, and accretion mechanisms are combined together and confronted with observations.This detailed review summarises the current knowledge on the theory and observations of winds from massive stars, as well as on observations and accretion processes in wind-fed high mass X-ray binaries. The aim is to combine in the near future all available theoretical diagnostics and observational measurements to achieve a unified picture of massive star winds in isolated objects and in binary systems.     

最大熵分位值估计及其对偶型优化解法

针对经典最大熵分位值估计中拉格朗日系数计算目前存在高度非线性、计算结果精度不高或有时难以收敛等问题,提出了一种对偶型 逐次寻优的方法.基于拉格朗日对偶法,推导建立了含有拉格朗日系数优化函数的对偶表达式;在此基础上,基于样本的概率权重矩约束,提出了逐次寻优算法.针对几种常见的概率分布类型和一种较为复杂的概率分布类型,采用对偶型最大熵方法和经典最大熵方法对其概率累积函数和分位值进行计算对比分析表明:对偶型最大熵分位值估计不仅具有非线性程度低、形式简单,而且对偶型 逐次寻优的方法具有比较高的计算精度,优化迭代的收敛性好等特点.      

球形收集极结构的二次电子产额测量装置及测量方法

为了精确测量材料在不同入射电子能量和入射电子角度下的二次电子产额(secondary electron yield, SEY)以及二次电子能谱,研制了收集极为球形结构的SEY测量装置。首先介绍了装置的构成、测量原理及中和方法,并对测得的信号波形进行了分析。随后,测量了Cu材料和Al₂O₃薄膜材料的SEY值和二次电子能谱。结果表明：不同入射电子能量下SEY值的标准偏差分别小于0.055(Cu)和0.126(Al₂O₃);不同入射电子角度下SEY值与理论模型符合的很好,拟合R²值为0.998 64(Cu);出射的二次电子能量绝大部分集中在10eV(Cu)和20eV(Al₂O₃)以下,符合相关理论预期。     

一种用于星载多波束相控阵的稀疏阵列

现有的技术较难满足星载多波束相控阵天线射频前端的通道间距,已有的研究工作大量集中在提高射频电路和芯片的集成度,提出采用稀疏布阵的方式来增加天线单元的平均间距,从而缓解现有技术条件下的高密度集成难题。设计了Ka频段八波束相控阵天线的稀疏布阵阵面,首先采用遗传算法优化设计64元稀疏子阵,子阵增益在±60°扫描范围内大于18.6dB,该子阵沿4个象限镜像对称,便于高效设计将不规则分布的天线单元端口与规则排布的R组件端口进行互连的带状线转接板,然后随机旋转、平移36个子阵拼接成全阵,在一定程度上打乱子阵分布均匀性,以起到栅瓣抑制的作用。该方法具有简单、高效、快捷的优点,稀疏阵列的设计结果基本能满足工程应用需求,适用于星载多波束相控阵。     

指数信号模型中参数的稳健估计

 给出了阻尼指数信号模型中参数的M 估计和Bootstrap M 估计; 基于Prony 方法给出估计的重新定义和新算法; 并且在较弱的条件下证明了这些估计的相容性; 最后利用Huber 函数给出了两种估计的模拟结果, 结果表明这两种估计的稳健性和精度都比传统的最小二乘估计好。     

具有独立失效模式的多自由度非线性振动系统的可靠性分析

 对不考虑失效模式相关性的多自由度非线性随机振动系统可靠性进行了研究。在结构系统响应和状态函数的前四阶矩的一般数学表达式的基础上,使用 Edgeworth级数把未知响应和状态函数的概率分布展开成标准的正态分布表达式,并放松了对随机参数的分布概型和激励类型的限制,从而确定了系统的可靠度。     

空/空机炮模态综合控制系统稳定性分析

在借鉴美国军用标准 MIL-F-8785C和 MIL-F-94 90 D的基础上 ,进行了综合飞行 /火力控制系统稳定性分析研究。以空 /空机炮模态为例 ,给出了综合控制系统小扰动稳定性分析准则 ,提出一种通过仿真计算得出系统稳定性指标的方法。最后以高性能控制仿真软件 MATRIXX6.0作为仿真平台进行了综合飞行/火力控制系统稳定性分析。实际应用表明 ,所提出的方法建模速度快、计算精度高、可靠性好 ,具有较强的实用性。